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The Sun II The Solar Atmosphere The Solar Wind The Solar Cycle.

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Presentation on theme: "The Sun II The Solar Atmosphere The Solar Wind The Solar Cycle."— Presentation transcript:

1 The Sun II The Solar Atmosphere The Solar Wind The Solar Cycle

2 Solar Granulation Careful observations of the base of the photosphere reveal “granulation” …a patchwork of dark and bright regions that are constantly changing Characteristic spatial extent of 700 km and lifetimes of 10 minutes This is the top of the convection zone protruding into the photosphere!!!! Absorption lines exhibit Doppler shifts indicating radial velocities of patches of about 0.4 km/s. The bright cells are vertically rising hot convective bubbles!!! When these bubble reach the optically thin photosphere they release their energy in the form of photons. The resulting cooler, darker gas sinks back into the interior

3 Solar Granulation

4 Differential Rotation Photospheric absorption lines may also be used to measure rotation rate of the sun at the solar limb At the equator the rotation period is approximately 25 days whereas at the poles the rotation period is approximately 36 days Solar rotation also varies with radius. At the “Tacholine” at about 0.7 R sun the rotation rates converge at the base of the convection zone The strong shear that is set up in this region is believed to result in electric current in the highly conducting plasma Probably the source of the Sun’s Magnetic Field!!!!!

5 The Chromosphere Intensity of only about 10 -4 of the value of the photosphere. Lies just above the photosphere and extends upward approximately 1600 km. Gas density drops by about 10 -4. Temperature increases from 4400 K to about 10,000K Additional lines that are not possible prevalent in the lower temperatures/higher pressures of the photosphere can be produced here. He-II, Fe-II Si-II, Cr-II Ca-II Some emission lines appear in addition to absorption lines particularly those wavelengths outside of the visible range. Some visible wavelength emission lines can be observed during a brief instant during eclipses Supergranulation and other structure is observed in the chromosphere. These are continued effects of the underlying convection zone Doppler studies indicate radial velocities of about 0.4 km/s Gas rising in the center of the supergranules and falling at the edges

6 The Chromosphere Spicules Spicules: Vertical filaments of gas extending upward from the chromosphere for 10,000 km Individual lifetime of about 15 minutes Several percent of the surface area of the Sun is covered by Spicules at any moment Material moving outward at speeds of 15 km/s

7 The Transition Region The region above the chromosphere with rapidly varying temperature that eventually reaches 100,000K over 100km. The temperature then slowly rises to about 1,000,000K The transition region can be observed in the Ultraviolet and extreme- ultraviolet regions of the spectrum Sun viewed in the extreme Ultraviolet http://umbra.nascom.nasa.gov/eit/

8 The Corona Visible during eclipses when the Moon fully occults the photosphere. Faint radiation nearly 10 6 times less intense than the photosphere Number density of particles at the base is 10 15 particles/m 3 (solar wind at 10 7 particles/m 3 ) Not in local thermodynamic equilibrium. Temperature means what?… T~2x10 6 K by some measures Low number densities allow forbidden transitions to occur Source of radio wavelength emission free-free electron transitions X-ray emission observed due to high temperature

9 The Corona

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11 Coronal Holes and the Solar Wind Images of the Sun in X-ray and extreme UV show that XUV and X-ray emission is not uniform X-ray bright Regions: Associated with the closed magnetic field lines that return to the Sun. Coronal holes: darker/cooler regions in X-ray emission –Localized bright spots can appear and disappear on the timescale of hours in the coronal holes –The weaker X-ray emission is characteristic of the lower temperatures and densities in the region of the holes –The existence of coronal holes is tied to the Sun’s magnetic field and the generation of a fast solar wind. –Magnetic field lines in these regions are believed to be “open”. Charged particles can “stream” along these “open” field lines and escape. Solar Wind: –Fast: a continuous stream of ions and electrons escaping from the Sun and moving through interplanetary space at ~ 750 km/s. –Slow: Gusty, about half of the speed 375/km/s. Produced by streamers in the Corona associated with closed magnetic fields SOHO Extreme UV image SOHO 3 X-ray band image

12 Magnetic Field of Sun Magnetic Field of Sun is significant. With high degree of spatial and temporal variability. Field strength at surface is typically 10 -4 T. “Open” field lines: Some of the magnetic field lines extend out for great distances from the Sun. Closed field lines: The magnetic field lines that directly return to the Sun. Solar Magnetic field interacts strongly with charge particles in its atmosphere via the Lorentz Force Charged particles are forced to spiral around the magnetic field lines (If E is negligible) Closed field lines tend to trap charged particles !!!! In regions of open field lines charged particles can follow the field lines out away from the Sun

13 Magnetic Field Lines Reconnection http://www.aldebaran.cz/astrofyzika/plazma/recon nection_en.htmlhttp://www.aldebaran.cz/astrofyzika/plazma/recon nection_en.html

14 Solar Wind

15 Comet Tails: Evidence for Solar wind even before solar wind particles directly detected. It is the electrical interaction between the ions of the solar wind and the ions in the ion tail that make the ion tail point directly away from the Sun. Aurora (Borealis/Australis): The ions from the Sun interact with the Earth’s magnetic field becoming trapped. These ions bounce back and forth between the poles forming the Van Allen Radiation Belt. The ions that are sufficiently energetic will collide with atoms in the upper atmosphere of the Earth causing the atoms to either become excited or ionized. It is these de- excitations and recombination that produce the light of the aurora. Direct Detection and Measurement: Ulysses spacecraft measured the solar wind at a distance of 1 AU from the sun (even out of the ecliptic plane). Speed 200 km/s - 750 km/s. Density 7 x 10 6 ions/m 3. Temperature 4 x 10 4 K for protons, 10 5 K for electrons.

16 Solar Wind how much?how far

17 Solar wind runs into interstellar wind …termination shock at 95 A Known as Heliopause http://voyager.jpl.nasa.gov/mission/interstellar.html

18 Making the assumption that the gas is isothermal we can integrate and obtain an expression for the number density (and pressure) as a function of radius: Where And n=n 0 at some radius r=r 0.  is approximately the ratio of a proton’s gravitational energy and its thermal kinetic energy at a distance r 0 from the Sun. The pressure can be written as: This pressure does not approach zero as At r 0 =1.4 R  T~1.5 x 10 6 K n 0 =3 x 10 13 m -3. ~5.5. The actual values are much lower….. Parker Wind Model How does expansion of the Corona produce the Solar wind? High thermal conductivity of the plasma in the Corona --> Almost Isothermal Consider Hydrostatic Equilbrium equation in region of Corona. M r ~M . Assuming that gas is completely ionized hydrogen From Ideal Gas Law we may write: The Hydrostatic equilibrium equation becomes:

19 In the solar atmosphere, the simple approximation of hydrostatic equilibrium must be replaced by a set of hydrodynamic equations that describe the flow. In particular when we write Equation 10.5 becomes Where v is the velocity of the flow. Conservation of mass flow can be expressed as This expression immediately implies that At the top of the convection zone, the motion of the hot, rising gas and the return flow of the cool gas sets up longitudinal (pressure) waves that propagate outward. Hydrodynamic Nature of the Upper Atmosphere The outward flux of wave energy can be expressed as: Where v s is the local sound speed and v w is the velocity amplitude of the oscillatory wave motion for individual particles being driven about their equilibrium positions by the “piston” of the convective zone. From Eq 10.84 the sound speed is given by Using the ideal gas law we can re-write this as

20 At the top of the convective zone v w v s as particles in the wave try to travel through the medium faster than a local speed of sound. Shock Wave Hydrodynamic Nature of the Upper Atmosphere Shock Front: A very steep density change over a short distance. As a shock moves through a gas it produces a great deal of heating through collisions, leaving the gas behind the shock highly ionized. This heating comes at the expense of the mechanical energy of the shock which quickly dissipates. Gas in Chromosphere is heated by the mass motions created in the convective zone!!! http://www.phy.ntnu.edu.tw/ntnujava/index.php?topic=21.0

21 Magnetohydrodynamics (MHD) and Alfven Waves MHD is the study of the interactions between magnetic fields and plasmas. Hydrodynamic equations discussed so far left out the effect of the Sun’s magnetic field. The temperature structure of the outer solar atmosphere is due at least in part to the presence of the magnetic field coupled with mass motions produced by the convective zone. The presence of a magnetic field allows for the generation of a 2nd type of wave motion. These waves propagate along the magnetic field lines as a consequence of the restoring force of the field lines. Magnetic Energy Density Magnetic field lines “frozen” into plasma Density of field lines and hence the magnetic field strength changes when a plasma is compressed in a direction perpendicular to the field lines. Energy density of B has increased Mechanical work was done, but Magnetic Pressure exists

22 A disturbance in the magnetic field line can propagate down the line… Alfven Wave Transverse MHD wave Speed of propagation can be estimated by comparing with sound speed in gas The Alfven wave speed should be approximately More careful treatment results in: Magnetohydrodynamics (MHD) and Alfven Waves Magnetic Pressure Gradient established when field lines are compressed This pressure change tends to push the field lines back, restoring the original density. Analagous to oscillations on a string when plucked. Tension on the string pulls it back… Magnetic Pressure Gradient “Tension”

23 Magnetohydrodynamics (MHD) and Alfven Waves Alfven waves may transport energy outward. Time-varying Magnetic field Electric Field Electric Current in Plasma Resistive Joule Heating Temperature rise

24 Alfven Waves and sound speed

25 Magnetohydrodynamics (MHD) and Alfven Waves http://en.wikipedia.org/wiki/Magnetohydrodynamics http://solar.physics.montana.edu/magara/Research/Topics/MHD_waves/mhdw.html http://sun.stanford.edu/~keiji/daily_mhd/daily_mhd.html

26 Alfven Waves http://link.brightcove.com/services/player/bcpid1513658585?bctid=1670022418 http://www.seas.columbia.edu/~ah297/un-esa/astrophysics/astro-chapter6.html

27 Solar Magnetic Field Sun Rotates Open B-field lines are dragged along through interplanetary space Solar Wind is forced to move with the field lines Torque Produced Sun’s rotation is slowed No apparent differential rotation in corona or solar magnetic field

28 The Outer Atmosphere of other Stars Looks like stellar winds slow down many stars rotations…even for low mass stars Wind transfering angular momentum away from star Late main sequence stars slower rotation rates than younger stars This Chandra image is the most detailed ever made of the remains of an exploded star. The one million-second image shows a bright outer ring ten light years in diameter that marks the location of a shock wave generated by the supernova explosion. A large jet-like structure protrudes beyond the shock wave in the upper left. Scale: Image is 8 arcmin per side. http://chandra.harvard.edu/photo/2004/casa/more.html Eta Carinae: HST image

29 The Solar Cycle Sunspots Number of Sunspots is periodic going from minimum to maximum and back to minimum in approximately 11 years The average latitude of sunspot formation also periodic with an ~ 11 year cycle. Individual sunspots are short-lived typically no longer than 1 month Individual sunspot remains at same latitude. Although succeeding sunspots are formed at progressively lower latitudes…hmmm? New cycle typically begins at +/- 40  Darkest portion known as the Umbra may measure as much as 30,000 km in diameter. Surrounded by the penumbra associated with magnetic lines of force. Zeeman effect splitting of spectral lines Strength of Magnetic Field Polarization of light Direction of Magnetic Field Field strengths of several 0.1 Tesla and greater have been measured in centers of Umbral Regions. Polarization indicates that field is vertical in center of umbra moving to horizontal at edges of penumbra Magnetic Fields Sunspots

30 How Sunspots are formed…The movie! http://soho.nascom.nasa.gov/gallery/Movies/10th/SunspotsForm.mov

31 Sunspots Generally located in groups. Lead sunspot will typically have one polarity. The lead sunspot in the other hemisphere will have opposite polarity. Trailing sunspots will have opposite polarity. During the next 11 year cycle the polarities will be reversed. Accompanying this local polarity reversal is a global polarity reversal. The overall dipole field of the sun will change so that magnetic north pole will switch from geographic north to south!!!! Polarity reversal always occurs during sunspot minimum. Polarity reversal has a 22-year cycle Dark Appearance due to relatively lower temperature. Central portion of Umbra may be as low as 3900K compared with 5777K. Factor of 4.8 reduction in flux. Most likely magnetic fields are inhibiting convective motion in the sunspot Much longer timescale variability as well. Maunder Minimum between 1645 and 1715 had a drastically reduced number of sunspots. (mini-ice age in Europe during this time). Resulting only from a few tenths percent reduction in solar energy output!!! Amount of carbon-14 related…can be tracked Magnetic Pressure believed to keep sunspot from sinking!!!

32 Polarity Reversal and Differential Rotation

33 The Solar Cycle Sunspots

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35 Solar Flare Eruptive events 10 17 J (lowest detectable) - 10 25 J of energy over tie intervals ranging from milliseconds to over an hour. (10 25 J = 317 million GW-yr) Large flares can be 100,000 km long. Hydrogen alpha emission lines visible. Radio-x-ray emission Charged particles ejected. Solar Cosmic Rays…mostly protons and helium nuclei…may reach earth in 30 minutes…dangerous to astronauts and disruptive to communications. Flares develop where magnetic field intensity is great…sunspot groups. Quick release of magnetic energy---> flare. Still a matter of active research.. Model of Solar flare involves reconnection of magnetic filed lines Solar Flare Model Disturbance in magnetic field loops Sheet of current in the highly conducting plasma Joule heating of gas Temperature rises to 10 7 K Particles Accelerated away from the reconnection point and away from the Sun may escape Solar Cosmic Rays Synchrotron Radio Emission, Soft X-ray from high temperatures below connection point

36 Solar Flare

37 Solar Flare Simulation http://ve4xm.caltech.edu/Bellan_plasma_page/laborato.htm

38 Solar Prominences Quiescent Prominence: Curtains of Ionized gas that reach well into the Corona and can remain stable for weeks or months. –The material in the prominence has collected along the magnetic filed lines of an active region. –The gas is cooler (8000K) and much more dense than the surrounding coronal gas. –This denser gas “rains” back down into the chromosphere. –When viewed in H  at the limb, the prominence appears as a bright structure against the thin Corona –When viewed in the continuum against the solar disk, a promincence appears as a dark filament absorbing light from below. Eruptive Prominence: may exist for a few hours and may develop abruptly from a quiescent prominence. A relatively stable magnetic field can suddenly become unstable. Prominence lifts away from the Sun!!! Related to solar flare Most of energy however goes into mass motions as gas is ejected instead of into EM radiation Coronal Mass Ejection: Routinely detected by SOHO instruments (daily on average). During periods of high sunspot activity up to 3.5 CME’s/day 5 x 10 12 -5 x 10 13 kg /CME 400 km/s to >1000 km/s Magnetic “bubble” lifting off of Sun after reconnection event

39 Masuda Solar Flare Model

40 Coronal Mass Ejection

41 How Sunspots, Flares and Coronal Mass Ejections are formed…

42 Magnetic Dynamo Theory Solar Cycle related to changing of magnetic field of the Sun Magnetic field lines “frozen” into plasma Differential Rotation Convection Differential Rotation Dragging of magnetic field lines Poloidal Toroidal Turbulent Convective Zone Twisting the lines creating regions of intense magnetic fields (ropes) Magnetic Pressure Buoyancy …Sunspot Groups

43 Magnetic Dynamo Theory Magnetic Dynamo theory explains many aspects of the Solar Cycle Latitude dependence of Sunspot development Magnetic Polarity of Sunspots Sun’s Polarity reversal Solar cycle period of 22 years Other stars Evidence for magnetic activity Observation of Starspots Still much to learn Relation to Earth’s Climate….

44 Plasmas http://www.plasma- universe.com/index.php/Plasma-Universe.comhttp://www.plasma- universe.com/index.php/Plasma-Universe.com

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51 March 7 2012 Solar Flare observed by FERMI in Gamma Rays


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